东天山北麓老奇台黄土中的孢粉化石

老奇台位于博格达山北坡开垦河冲、洪积扇中部。山麓地区黄土呈带状广泛分布,平行于山脉走向,东西绵延约200公里,南北宽约25公里,覆盖于不同时代地层之上。厚度从2—30米不等,一般为土黄色粉砂质粘土,细而均匀,富含碳酸盐类。黄土分布的上限往往与云杉林分布的下限相一致,海拔为1700米左右。当地1700米—2700米的中山带现广布雪岭云杉林,海拔1500米—1700米的山地河谷内是桦、山杨、榆等阔叶落叶树与云杉形成的混交     

Calculations concerning interstellar isomeric abundance ratios for C3H and C3H2

The syntheses of interstellar c-C3H2, H2CCC, c-C3H, and HCCC, where "c" stands for the cyclic isomer, are thought to proceed via dissociative recombination of the precursor ions c-C3H3+ and H2CCCH+, which are themselves produced mainly via the radiative association reaction between C3H+ and H2. We have utilized ab initio methods to study the potential energy surface (PES) for the association of the linear ion C3H+ and H2 to form the isomers c-C3H3+ and H2CCCH+. The overall rate coefficient for radiative association has been calculated as a function of temperature via the phase space method. Our ab initio calculations show that the H2CCCH+ isomer is formed directly without an activation barrier from reactants, and that isomerization between the two isomers can occur readily via a low-energy pathway consisting of two transition states (saddle points on the PES) and one intermediate (local minimum on the PES). Calculations of the equilibrium coefficient for the isomerization H2CCCH+ <-> c-C3H3+ as a function of energy shows that equal abundances of these two ions should be produced as relaxation proceeds, in agreement with experimental measurements at high pressure. Our results confirm the important point that a simple ion-molecule association reaction can produce a cyclic hydrocarbon. If dissociative recombination reactions involving c-C3H3+ and H2CCCH+ maintain the carbon skeletal structure of the ions and produce roughly similar C3H/C3H2 branching ratios, then abundance ratios of unity are produced between the cyclic and noncyclic isomers of C3H and C3H2 via this mechanism. The large abundance ratio of c-C3H2 to H2CCC observed in TMC-1 can then be explained by differential destruction rates.     

The 825-1110 angstroms EUV spectrum of Venus

On 15 August 1994 we launched the EUVS sounding rocket payload to observe the 825-1110 angstrom region of Venus's far ultraviolet airglow spectrum. The EUVS telescope/spectrograph obtained good data at five times higher spectral resolution than was previously available in the far ultraviolet. We present these data and compare our results to those obtained by the Galileo UVS and Venera 11/12 UV spectrophotometers. We identify several new spectral emission features, including both singly ionized nitrogen and molecular nitrogen in Venus's spectrum. We also see evidence for electron-impact-induced emission from CO. Finally, the EUVS data indicate that the "Ar" emissions detected in Venus's far ultraviolet spectrum by Venera 11/12 spectrophotometers are in fact not due to argon, thus eliminating the discrepancy between in situ and remote sensing measurements.     

混合海气耦合模式的研制和El Ni?o的预告试验

所使用的海气耦合模式是由COLA R15 AGCM和简单的CZ海洋模式耦合而成。使用该混合海气耦合模式完成了15次ENSO试验预报,预告和观测的Ni?o 3指数超前15个月的相关系数达0.6（在0.01有意义水平上该相关系数在统计上是有意义的）,超前一年半的Ni?o 3指数的预告误差大约为0.6～0.9℃。预告结果表明混合海气耦合模式具有预测ENSO的能力达15个月。最后,还讨论了该模式的优点和进一步改进的途径。